All Figures

Figure 1: Comparison of the 101 modelled PNe with the evolutionary tracks in the HR diagram. The model black-body temperatures are plotted against the luminosities interpolated from tracks. Filled circles indicate [WR] stars, open circles are wels and pluses indicate non-emission-line stars. The dotted lines show H-burning evolutionary models of Blöcker (1995), labeled by mass in units of . The solid lines are isochrones, labeled by the time after the nebula ejection, in units of 103 yr.

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In the text

	Figure 2: The CSPN mass histograms. Upper panel: the histogram of all modelled PNe. Lower panel: the histogram of different subgroups of the 101 PNe. The dashed line indicates [WR] stars, the dotted line wels and the solid line non-emission-line stars.
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In the text

	Figure 3: The mass distribution of non-emission-line O-type CSPNe (shaded area) is compared to two DA white dwarf distributions of intermediate temperatures: thin line: data from Liebert et al. (2005); dotted line: data from Madej et al. (2004) which are more numerous, and are rescaled.
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In the text